Solnechno-Zemnaya Fizika Solnechno-Zemnaya Fizika Солнечно-земная физика 2712-9640 27729 10.12737/szf-52201901 14-я Китайскo-Российская конференция по космической погоде. Хайкоу, Китай, 5–9 ноября 2018 г. 14th China-Russia Space Weather Workshop. November 5–9, 2018, Haikou, China 14-я Китайскo-Российская конференция по космической погоде. Хайкоу, Китай, 5–9 ноября 2018 г. Fine structure events in microwave emission during solar minimum События с тонкой структурой в микроволновом излучении во время солнечного минимума Чэнмин Тань Chengming Tan tanchm@nao.cas.cn Биолинь Тань Baolin Tan bltan@nao.cas.cn Ихуа Янь Yihua Yan Вэй Ван Wei Wang wwang@nao.cas.cn Линьцзе Чэнь Linjie Chen ljchen@nao.cas.cn Фэй Лю Fei Liu feiliu@nao.cas.cn Ицзян Доу Yujiang Dou douyj@suda.edu.cn Национальные астрономические обсерватории Китая Пекин Китайская Народная Республика National Astronomical Observatories of Chinese Academy of Sciences Beijing China Университет Китайской академии наук Пекин Китайская Народная Республика University of Chinese Academy of Sciences Beijing China Национальные астрономические обсерватории Китая Пекин Китайская Народная Республика National Astronomical Observatories of Chinese Academy of Sciences Beijing China Университет Китайской академии наук Пекин Китайская Народная Республика University of Chinese Academy of Sciences Beijing China Главная лаборатория исследования солнечной активности, Национальные астрономические обсерватории, Академия наук КНР Пекин Китайская Народная Республика Key Laboratory of Solar Activity, National Astronomical Observatories, Chinese Academy of Sciences Beijing China Университет Китайской академии наук Пекин Китайская Народная Республика University of Chinese Academy of Sciences Beijing China Национальные астрономические обсерватории Китая Пекин Китайская Народная Республика National Astronomical Observatories of Chinese Academy of Sciences Beijing China Национальные астрономические обсерватории Китая Пекин Китайская Народная Республика National Astronomical Observatories of Chinese Academy of Sciences Beijing China Национальные астрономические обсерватории Китая Пекин Китайская Народная Республика National Astronomical Observatories of Chinese Academy of Sciences Beijing China Университет Сучжоу Сучжоу Китайская Народная Республика Soochow University Suzhou China 5 2 4 10 https://naukaru.ru/en/nauka/article/27729/view

Солнечный минимум представляет собой период, для которого характерно несколько меньшее количество солнечных пятен и эрупций. Раньше этому периоду уделялось меньше внимания. Поскольку радиосигнал быстро откликается на изменение солнечной плазмы и магнитного поля, мы провели комплексный анализ спектральных данных высокого разрешения, полученных SBRS и MUSER: 1) поиск солнечных радиовсплесков различных ви-дов за последние солнечные минимумы (2007–2009 и 2016–2018 гг.); 2) анализ нескольких типичных радиовсплесков, отрицательного и положительного дрейфующих всплесков, например, события, про-изошедших 22.11.2015 и 29.08.2016, событий со сверхтонкой спектральной структурой с мини-вспышкой и даже без солнечных пятен, например, событий, зарегистрированных 28.03.2008. и 04.07.2017. Эти результаты показали, что во время солнечных минимумов было много радиовсплесков с тонкой структурой. Эти события происходили не только в мощных вспышках, но и в слабых (класс C и B по GOES) или даже без вспышек, но в областях, связанных со слабым уярчением или выбросом. Мы полагаем, что слабые солнечные радиовсплески, наблюдаемые телескопами с высокой чувствительностью и низкой интерференцией, помогут нам понять основные физические характеристики мелкомасштабных солнечных эрупций.

The solar minimum is a period with a relatively smaller number of sunspots and solar eruptions, and has been less studied before. Since the radio signal rapidly responds to the change of solar plasma and magnetic field, we perform a comprehensive analysis of high resolution spectrum data from SBRS and MUSER: 1) a search for solar radio bursts of different kinds in recent solar minima (2007–2009 and 2016–2018); 2) an analysis of several typical radio burst events, negative and positive drifting bursts, for example the November 22, 2015 and August 29, 2016 events; superfine spectral structure events with mini-flares and even without sunspots, for example the March 28, 2008 and July 04, 2017 events. These results show that there were many radio bursts with a fine structure during solar minima. These events occurred not only in powerful flares, but also in faint flares (class C and B by GOES) or even without flares, but in regions related to weak brightenings or ejecta. We assume that the weak solar radio bursts observed by telescopes with high sensitivity and low interference will help us to understand the basic physical characteristics of small-scale solar eruptions.

 солнечный минимум вспышка радиовсплеск спектр тонкая структура solar minimum flare radio burst spectrum fine structure

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